The flux density values for phase calibrators were determined using the task FLUXSCALE in CASA. The calibration solutions were applied to the multi-source datasets and visibility data for individual targets were extracted using the CASA task SPLIT while averaging the spectral channels to account for bandwidth smearing effects. The Stokes I images of our sources were created using the multiterm-multifrequency synthesis [1]} algorithm in CASA task TCLEAN. This was followed by four rounds of phase-only self-calibration and five rounds of amplitude and phase self-calibration. The Stokes Q and U images were created using the final self-calibrated visibility data. We used same imaging parameters as for the Stokes I image except for lesser number of iterations.
